Galaxy Survey data analysis using SDSS-III as an example

Transcription

1 Galaxy Survey data analysis using SDSS-III as an example Will Percival (University of Portsmouth) showing work by the BOSS galaxy clustering working group"

2 Cosmology from Spectroscopic Galaxy Surveys" What are the constituents of matter?" What is the physics of inflation?" e.g. neutrino mass, primordial P(k)" Galaxy Redshift" Survey" Redshift-space distortions" What is the expansion rate of the Universe?" e.g. quintessence, Λ" How does structure form within this background?" e.g. modified gravity, GR" Understanding " acceleration" Is the Universe homogeneous " on large scales?" Copernican principle, Non-Gaussianity" Other non-cosmology science" e.g. galaxy formation & evolution"

16 Redshift failures & close pairs" Spectra where we failed to get an accurate redshift are spatially correlated" Close pairs obviously correlated with density" Correct both by upweighting the nearest target with good classification " Ross et al."

29 Key BAO measurements" ξ(r) and P(k) based es.ma.ons are appropriate and unbiased, but they include the noise from small scales and shot noise differently We average the two results, and compute the error bar using the observed sca2er of the average value in the mocks. This shows no significant departure from a Gaussian distribu.on Anderson et al."

30 CMASS results" Anderson et al."

31 Extra information from additional measurements" Including the quadrupole allows us to measure H and d A separately (or include an additional measurement of F) " F = (1+z) d A (z)h(z)/c " F called the Alcock-Paczynski parameter " Measure the growth rate from the peculiar velocities through redshift-space distortions" fσ 8 (z=0.57)" amplitude of velocity field" See a wide variety of physics from the full shape of the clustering statistic (as a function of scale)" Ω m, Ω b, Ω ν, f NL, n s!

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